67 Aquarii

67 Aquarii is a star located 484[1] light years away from the Sun in the zodiac constellation of Aquarius. 67 Aquarii is its Flamsteed designation.[9] It is a dim, blue-white hued star near the lower limit of visibility to the naked eye with an apparent visual magnitude of 6.40.[2] At the distance of this star, its visual magnitude is diminished by an extinction of 0.11 due to interstellar dust.[8] The position of this star near the ecliptic means it is subject to lunar eclipses.[10]

67 Aquarii
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Aquarius
Right ascension  22h 43m 14.26269s[1]
Declination −06° 57′ 46.5752″[1]
Apparent magnitude (V) 6.40[2]
Characteristics
Evolutionary stage main sequence[3]
Spectral type B7.5 V[4] or B9 V[5]
B−V color index −0.039±0.008[2]
Astrometry
Radial velocity (Rv)2.0±3.8[2] km/s
Proper motion (μ) RA: +26.147[1] mas/yr
Dec.: −10.192[1] mas/yr
Parallax (π)8.0002 ± 0.0694[1] mas
Distance408 ± 4 ly
(125 ± 1 pc)
Absolute magnitude (MV)1.12[2]
Details
Mass2.46±0.05[3] M☉
Radius2.0[6] R☉
Luminosity41.9+5.5
−4.9[3] L☉
Surface gravity (log g)3.998±0.014[7] cgs
Temperature10,257±48[3] K
Rotational velocity (v sin i)205[3] km/s
Age316[8] Myr
Other designations
67 Aqr, BD−07°5838, FK5 3819, GC 31703, HD 215143, HIP 112179, HR 8647, SAO 146273[9]
Database references
SIMBADdata

This is a late B-type main-sequence star with a stellar classification of B7.5 V,[4] which indicates it is generating energy through hydrogen fusion at its core. It is 316[8] million years old and is spinning rapidly with a projected rotational velocity of 205 km/s;[3] the critical velocity for this star is 377 km/s.[7] 67 Aquarii has 2.46[3] times the mass of the Suns and about double the Sun's radius.[6] It is radiating 42[3] times the luminosity of the Sun from its photosphere at an effective temperature of 10,257 K.[3]

References
  1. Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015.
  3. Zorec, J.; et al. (2012), "Rotational velocities of A-type stars. IV. Evolution of rotational velocities", Astronomy and Astrophysics, 537: A120, arXiv:1201.2052, Bibcode:2012A&A...537A.120Z, doi:10.1051/0004-6361/201117691.
  4. Hube, Douglas P. (1970), "The radial velocities of 335 late B-type stars", Memoirs of the Royal Astronomical Society, 72: 233–280, Bibcode:1970MmRAS..72..233H.
  5. Houk, N.; Swift, C. (1999), "Michigan catalogue of two-dimensional spectral types for the HD Stars", Michigan Spectral Survey, 5, Bibcode:1999MSS...C05....0H.
  6. Pasinetti Fracassini, L. E.; et al. (February 2001), "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS)", Astronomy and Astrophysics (Third ed.), 367 (2): 521–524, arXiv:astro-ph/0012289, Bibcode:2001A&A...367..521P, doi:10.1051/0004-6361:20000451.
  7. Huang, Wenjin; et al. (October 2010), "A Stellar Rotation Census of B Stars: From ZAMS to TAMS", The Astrophysical Journal, 722 (1): 605–619, arXiv:1008.1761, Bibcode:2010ApJ...722..605H, doi:10.1088/0004-637X/722/1/605.
  8. Gontcharov, G. A. (November 2012), "Spatial distribution and kinematics of OB stars", Astronomy Letters, 38 (11): 694–706, arXiv:1606.09028, Bibcode:2012AstL...38..694G, doi:10.1134/S1063773712110035.
  9. "67 Aqr". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-05-18.
  10. Edwards, D. A.; et al. (April 1980), "Photoelectric observations of lunar occultations. XI.", Astronomical Journal, 85: 478–489, Bibcode:1980AJ.....85..478E, doi:10.1086/112700. For example, see SAO 146273 on p. 482
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.